Hemispherical power asymmetry from scale-dependent modulated reheating

McDonald, John

doi:10.1088/1475-7516/2013/11/041

Cited by 22 publications

(22 citation statements)

References 42 publications

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“…The calculation is reviewed in our appendix A, where the correspondence between these calculations will be very clear. 9 Just before we accomplish the second version of this paper, we found a peper [36] in which a similar idea has been examined.…”

Section: Curvaton and Other Modulation Mechanisms (Multi-b)mentioning

confidence: 95%

Scale-dependent CMB asymmetry from primordial configuration

Kohri

Lin

Matsuda

2014

J. Cosmol. Astropart. Phys.

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We demonstrate that a topological defect can explain the hemispherical power asymmetry of the CMB. The first point is that a defect configuration, which already exists prior to inflation, can source asymmetry of the CMB. The second point is that modulation mechanisms, such as the curvaton and other modulation mechanisms, can explain scale-dependence of the asymmetry. Using a simple analysis of the δN formalism, we show models in which scale-dependent hemispherical power asymmetry is explained by primordial configuration of a defect.

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Section: Curvaton and Other Modulation Mechanisms (Multi-b)mentioning

confidence: 95%

Scale-dependent CMB asymmetry from primordial configuration

Kohri

Lin

Matsuda

2014

J. Cosmol. Astropart. Phys.

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“…Equation (25) implies that the comoving curvature perturbation R c ≡ H δφ φ 0 − is conserved outside the Hubble horizon. The comoving curvature perturbation R c is the same as that in the standard inflation model.…”

Section: The Conserved Quantity At Horizon Crossingmentioning

confidence: 99%

“…Several anisotropic inflationary models have been built to solve the power asymmetry problem [23][24][25][26][27][28][29][30]. Usually, the background spacetime of the anisotropic inflation model is described by Bianchi spacetime [31].…”

Section: Introductionmentioning

confidence: 99%

Finslerian dipolar modulation of the CMB power spectra at scales $$2<l<600$$ 2 < l < 600

Lin

2017

Eur. Phys. J. C

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A common explanation for the CMB power asymmetry is to introduce a dipolar modulation at the stage of inflation, where the primordial power spectrum is spatially varying. If the universe in the stage of inflation is Finslerian, and if the Finsler spacetime is non-reversible under parity flip, x → −x, then a three dimensional spectrum which is a function of wave vector and direction is valid. In this paper, a three dimensional primordial power spectrum with preferred direction is derived in the framework of Finsler spacetime. It is found that the amplitude of dipolar modulation is related to the Finslerian parameter, which in turn is a function of wave vector. The angular correlation coefficients are presented, and the numerical results for the anisotropic correlation coefficients over the multipole range 2 < l < 600 are given.

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“…Generalizations of P ζ will be considered in future work. 2 This is true, for example, for the modulated reheating model of [12], which also predicts no running of n σ .…”

mentioning

confidence: 91%

Hemispherical power asymmetry from a space-dependent component of the adiabatic power spectrum

McDonald

2014

Phys. Rev. D

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The hemispherical power asymmetry observed by Planck and WMAP can be interpreted as due to a spatially-varying and scale-dependent component of the adiabatic power spectrum. We derive general constraints on the magnitude and scale-dependence of a component with a dipole spatial variation. The spectral index and the running of the spectral index can be significantly shifted from their inflation model values, resulting in a smaller spectral index and a more positive running. A key prediction is a hemispherical asymmetry of the spectral index and of its running. Measurement of these asymmetries can test the structure of the perturbation responsible for the cosmic microwave background power asymmetry.

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Hemispherical power asymmetry from scale-dependent modulated reheating

Cited by 22 publications

References 42 publications

Scale-dependent CMB asymmetry from primordial configuration

Scale-dependent CMB asymmetry from primordial configuration

Finslerian dipolar modulation of the CMB power spectra at scales $$2<l<600$$ 2 < l < 600

Hemispherical power asymmetry from a space-dependent component of the adiabatic power spectrum

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